A model spectrum was computed by integrating the image fluxes at each wavelength.
At low inclinations it shows a single peaked profile with a shallow absorption feature in the red wing, caused by infalling optically thick gas obscuring part of the stellar surface and the shock region. This inverse P Cygni profile, which is considered to be a characteristic feature of hot hydrogen emission lines produced in accretion columns observed at face-on configurations [1]}, is visible in the model up to inclinations of 54\(^{\circ }\)  at velocities of 150 km/s up to 200 km/s, see Fig. REF .
At the lowest modelled inclination of 5\(^\circ \) , the emission line extends over a velocity range of about \(\pm \)  150 km/s, whereas beyond 54\(^\circ \) , the profile becomes double peaked and the range expands to \(\pm \)  220 km/s.
